High
resolution
Cluster
set
/
Large
filament
Simulation
Hutt/Leia is a set of 10 high resolution re-simulations of galaxy
clusters taken from a large size cosmological simulation using the
ZIC technique. In total there are 37 Halos with masses larger than
0.5e14 Msol/h, of which 6 have masses above 1.0e15 Msol/h. The initial
conditions where created to have a large (typical 5 R_200) region around
the objects, which is free from boundary effects. The g696 simulation (e.g. Leia)
cover even a region around a massive filament. These simulations include
various treatments of physical processes, some of them including radiative
cooling, star formation and feedback.
For a detailed information on the simulation set see
Dolag et al. 2009, MNRAS 399, 497 for the
individual clusters as well as Dolag et al. 2006
for the region containing the filament.
There are 92 simulation outputs. A list relating the snapshot number to the according redshift can be found
here.
Online services
Here are listed services which allows to browse the result of the simulations and obtain on the fly
results from the simulations. Some services are restricted to registered users only. Please
contact Gerard Lemson (lemson@mpa-garching.mpg.de) to obtain a user id.
Please also see here to how to give credits for the results you obtain.
List of Clusters
Name |
Pictures |
Halos |
|
|
|
ID |
Mass [Msol/h] |
g676 |
|
|
a |
1.1e14 |
g914 |
|
|
a |
1.3e14 |
g1542 |
|
|
a |
1.1e14 |
g3344 |
|
|
a |
1.1e14 |
g6212 |
|
|
a |
1.1e14 |
g1 |
|
|
a |
1.5e15 |
b |
4.8e14 |
c |
1.8e14 |
d |
1.6e14 |
e |
8.0e13 |
f |
5.6e13 |
g8 |
|
|
a |
2.3e15 |
b |
1.3e14 |
c |
9.6e13 |
d |
9.4e13 |
e |
8.6e13 |
f |
5.8e13 |
g |
5.3e13 |
g51 |
|
|
a |
1.3e15 |
g72 |
|
|
a |
1.4e15 |
b |
2.0e14 |
g696 |
|
|
a |
1.3e15 |
b |
1.2e15 |
c |
8.4e14 |
d |
7.4e14 |
e |
4.3e14 |
f |
2.5e14 |
g |
1.9e14 |
h |
1.8e14 |
i |
1.7e14 |
j |
1.6e14 |
k |
1.6e14 |
l |
1.5e14 |
m |
1.2e14 |
n |
9.0e13 |
o |
8.9e13 |
p |
8.0e13 |
q |
7.8e13 |
r |
7.6e13 |
s |
7.3e13 |
t |
7.3e13 |
u |
6.7e13 |
v |
6.1e13 |
w |
5.4e13 |
x |
5.4e13 |
y |
5.2e13 |
z |
5.2e13 |
# |
5.1e13 |
Included physics
- dm: dark matter only simulations
- ovisc: non radiative simulations (old scheme for viscosity is used, like in Gadget-1)
- svisc: non radiative simulations (new, signal velocity based viscosity, like in Gadget-2)
- lvisc: non radiative simulations (using time dependent viscosity scheme)
- csf: Radiative runs with star formation and "low" galactic winds (e.g. 350 km/s)
- csfsw: Radiative runs with star formation and "high" galactic winds (e.g. 480 km/s)
- csfnw: Radiative runs with star formation and "no" galactic winds
- csfc: Radiative runs with star formation, "low" galactic winds and thermal conduction (e.g. 1/3 of the spitzer value)
- m1: Radiative runs with star formation using metal enrichment
- mhd_z: non radiative simulations including magnetic fields
Simulation Parameters
Parameter used |
|
|
|
|
z_ini |
m_dm [Msol/h] |
f_bary [%] |
0.7 |
0.3 |
0.7 |
0.9 |
60 |
1.3e9 |
13 |
Some Papers using these cluster simulations:
-
Substructures in hydrodynamical cluster simulations,
Dolag, K.; Borgani, S.; Murante, G.; Springel, V.
-
The baryon fraction in hydrodynamical simulations of galaxy clusters,
Ettori, S.; Dolag, K.; Borgani, S.; Murante, G.
-
The impact of gas physics on strong cluster lensing,
Puchwein, E.; Bartelmann, M.; Dolag, K.; Meneghetti, M.
-
Simulated X-ray galaxy clusters at the virial radius: Slopes of the gas density,
temperature and surface brightness profiles,
Roncarelli, M.; Ettori, S.; Dolag, K.; Moscardini, L.; Borgani, S.; Murante, G.
-
Sunyaev-Zel'dovich profiles and scaling relations: modelling effects and observational biases,
Bonaldi, A.; Tormen, G.; Dolag, K.; Moscardini, L.
-
Thermal Conduction in Simulated Galaxy Clusters,
Dolag, K.; Jubelgas, M.; Springel, V.; Borgani, S.; Rasia, E.
Contact
Contact Klaus Dolag (kdolag@mpa-garching.mpg.de) in case of questions.